Here, two simulations have been performed with the Wagoner rate and our new rate of the \(^7\) Be(\(n\) ,\(\alpha \) )\(^4\) He reaction studied, respectively. It shows that
the predicted abundances of D, \(^3\) He and \(^4\) He do not change appreciably, while that for \(^7\) Li increases 1.2% by adopting the new rate. Therefore, the
present rate even worsens the \(^7\) Li problem. In order to clarify the reason, we have performed the reaction flux [1]} calculations. Figure REF 
shows the flow passing though arbitrary reaction involved in the BBN network in a timescale of about 10000 s (long enough for BBN) with the present rate. The
flux passing through the \(^7\) Be(\(n\) ,\(\alpha \) )\(^4\) He channel is about 10\(^{-12}\)  mol/g (marked by a dashed red arrow), which is about a factor of ten weaker than
the result using the Wagoner rate. Based on the present estimation, the role of \(^7\) Be(\(n\) ,\(\alpha \) )\(^4\) He in destroying \(^7\) Be is weakened from the secondary
importance to the third, and thus the \(^7\) Be(\(d\) ,\(p\) )2\(^4\) He reaction becomes the secondary important reaction in destructing \(^7\) Be.
In addition, our calculation shows that the cosmological \(^7\) Li problem could be solved (within the observation uncertainties) provided only if that the
thermonuclear rate of \(^7\) Be(\(n\) ,\(\alpha \) )\(^4\) He is about 180 times larger than the Wagoner rate under the condition of without changing the rates for those
rest reactions. Therefore, it is unlikely to solve the \(^7\) Li problem by a further study of this reaction.
